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Interstellar Extinction in the Direction of the Aquila Rift

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Interstellar Extinction in the Direction of the Aquila Rift A&A 405, 585–590 (2003) Astronomy DOI: 10.1051/0004-6361:20030599 & c ESO 2003 Astrophysics Interstellar extinction in the direction of the Aquila Rift V. Straiˇzys1,K.Cernisˇ 1, and S. Bartaˇsi¯ut˙e1;2 1 Institute of Theoretical Physics and Astronomy, Vilnius University, Goˇstauto 12, Vilnius 2600, Lithuania e-mail: [email protected] 2 Astronomical Observatory of Vilnius University, Ciurlionioˇ 29, Vilnius 2009, Lithuania e-mail: [email protected] Received 28 February 2003 / Accepted 14 April 2003 Abstract. The distance dependence of interstellar extinction in the direction of the Aquila Rift is investigated using 473 stars observed in the Vilnius photometric system. The front edge of the dark clouds in the area is found to be at 225 55 pc and ± the thickness of the cloud system is about 80 pc. The maximum extinction AV in the clouds is close to 3.0 mag. Two stars with larger extinction are found and discussed. Since the new distance of the clouds is larger than the previously accepted distance, the cloud system mass should be increased to 2:7 105 M which is close to the virial mass estimated from the CO velocity × dispersion. Additional arguments are given in favor of the genetic relation between the Serpens and the Scorpio-Ophiuchus dark clouds. Key words. stars: fundamental parameters – ISM: dust, extinction – ISM: clouds – ISM: individual objects: Aquila Rift – ISM: individual objects: Serpens molecular cloud 1. Introduction Stars and other sources in the area have been well cov- ered by the infrared surveys: by IRAS in the far infrared and Starting from Cygnus, in the direction of the Galactic center the by 2MASS in the JHK range. Also, numerous radioastronom- Milky Way appears to split into two branches. The southern ical studies in the lines of H I, CO, H2CO, NH3 and H2Oare branch runs through Cygnus, Vulpecula, Sagitta, Aquila and available in the area. The distribution of molecules, especially Scutum, entering the Galactic central bulge in Sagittarius. The of CO, shows a very close resemblance to the dust distribu- northern branch crosses Vulpecula and Aquila and disappears tion (see Dame & Thaddeus 1985; Dame et al. 1987, 2001). in the northern part of the Serpens Cauda and Ophiuchus con- According to CO radio observations, the Aquila Rift occupies stellations, being covered by numerous dust clouds. This com- a region of irregular form between 20◦ and 40◦ in Galactic lon- plex of dark clouds usually is called the Aquila Rift. gitude and between –6◦ and +14◦ in Galactic latitude. However, The distances and extinction properties of these clouds are some protrusions and blobs of gas and dust extend up to ` = 15◦ known only with low accuracy. So far the area is poorly inves- and b =+20◦. tigated by modern photometric methods in the optical range. About a decade ago we started a program of investiga- The collected UBV and MK data have been used for a crude es- tion of the Serpens Cauda clouds belonging to the Aquila timate of the dependence of interstellar extinction on distance Rift by photoelectric photometry of stars in the Vilnius seven- in the Rift direction (FitzGerald 1968; Neckel & Klare 1980; color photometric system (Table 1). Our first results were Forbes 1985 and others). A sudden appearance of reddened published by Straiˇzys et al. (1996), hereafter Paper I. The in- stars at 200–250 pc is observed. According to the summary of vestigation was based on photometry and photometric classifi- Dame & Thaddeus (1985), the estimated distance of the Aquila cation of 105 stars down to magnitude 13, located around the Rift is 200 100 pc. ± core of the Serpens molecular cloud mentioned above. The size A field around the core of one of the densest Serpens molec- of the area investigated was about 6.5 square degrees. It was h m ular clouds (at 18 30 , +1◦14.50, 2000.0) with active star for- found that the dust cloud in the area appears at a distance of mation has attracted more attention (see the review article by about 260 pc. Eiroa 1991). The distance of the cloud has been discussed by However, the area investigated in Paper I is only a small Strom et al. (1974), Chavarria et al. (1987, 1988), Zhang et al. part of the whole complex of the Aquila Rift. The newest cat- (1988), de Lara & Chavarria (1989), de Lara et al. (1991) and alog of dark clouds of Dutra & Bica (2002) enumerates in the Straiˇzys et al. (1996). Rift more than 50 clouds of different sizes. It is important to know whether all these clouds are at the same distance or they Send offprint requests to:V.Straiˇzys, e-mail: [email protected] form a system with a significant depth. Article published by EDP Sciences and available at http://www.aanda.org or http://dx.doi.org/10.1051/0004-6361:20030599 586 V. Straiˇzys et al.: Interstellar extinction in the Aquila Rift Fig. 1. The chart for the investigated Serpens Cauda area with the following sub-areas: A is the sub-area investigated in Paper I; Ser I, Ser II, Ser III and Ser IV are the sub-areas in which photoelectric standards have been measured for future CCD photometry (Cernisˇ et al. 1997 and Paper III); SA 110 is the area in which HD stars have been measured by Zdanaviˇcius et al. (1978). The broken line at RA = 18h19m divides the area into two parts with different dependence of AV on distance. Table 1. Mean wavelengths and half-widths of passbands of the in Table 2. The measured stars in the sub-areas I–IV will be Vilnius photometric system. used as standards for future CCD photometry of fainter stars. Kapteyn Selected Area 110 is located at the edge of the same Passband UP X Y Z VS area. In it Vilnius photometry of 30 HD stars has been published by Zdanaviˇcius et al. (1978). These stars were also included λ (nm) 345 374 405 466 516 544 656 in the present study of interstellar extinction (see Table 2). ∆λ (nm) 40 26 22 26 21 26 20 Magnitudes and color indices of stars in the sub-areas are pub- lished in the papers listed in Table 2. Table 2. Four sub-areas in which fainter stars have been measured in In the present study the extinction data of 80 stars from the Vilnius photometric system and SA 110. Paper I were also used. Their distances are transformed to the new distance scale corresponding to the distance modulus of Sub- RA Dec Magnitude Number Publ. Hyades V MV = 3:3. Other stars of Paper I were rejected: area h m limits of stars − ◦0 some of them were found to be visual binaries and for some Ser I 18 01.3 –00 18 11.3–14.4 11 1 the classification accuracy from the photometric data was too Ser II 18 31.5 –00 50 11.0–13.4 4 2 low. They are either unresolved binaries or peculiar objects. Ser III 18 32.5 –01 23 10.2–12.5 7 2 Consequently, we had at our disposal photometry of about Ser IV 18 39.0 +00 10 8.0–13.3 45 2 600 stars in total (14 stars are common to the catalogs of SA 110 18 46.5 –01 00 6.9–10.7 30 3 Papers I and II and 8 stars are common to the catalogs of Paper II and SA 110). However, for the investigation of extinc- Publications: (1) Cernisˇ et al. (1997), (2) Straiˇzys et al. (2002c, tion in the area we used 473 stars only, after the exclusion of Paper III), (3) Zdanaviˇcius et al. (1978). binary, multiple and peculiar stars. The map of the investigated area with the sub-areas is shown in Fig. 1. In the present paper we investigate interstellar extinction and cloud distances in a much larger area, covering 5 2. Interstellar extinction law 10 sq. degrees. The area is limited by the following 2000.0 co-× h m h m ordinates: RA from 18 00 to 18 48 and DEC from 3:0◦ We have identified 43 stars from our list with the 2MASS sur- − to +2.0◦. Photometry in the Vilnius system was obtained vey photometry available through the Internet (Skrutskie et al. in 1994, 1997 and 2001 with the 1 m telescope at the 1997). For 19 stars, covering the range of extinctions AV Maidanak Observatory in Uzbekistan. The results of photom- from 0.4 to 2.5 mag, we have calculated color indices V K − etry of 419 stars down to 11 mag and their photometric clas- taking V from Table 1 of Paper II, and color excesses EV K tak- − sification were published by Straiˇzys et al. (2002b), hereafter ing the intrinsic (V K)0 from Straiˇzys (1992, Tables 22–24). Paper II. Spectral types of these− stars were taken from spectroscopic Additionally, 67 fainter stars with V between 10th classification. The least squares solution gives the equation: and 14th mag were observed in four smaller sub-areas situated within the large area indicated above. These sub-areas are listed EV K=EY V = 3:295 + 0:347 (Y V)0 0:464 : (1) − − − ± V. S t r a izys ˇ et al.: Interstellar extinction in the Aquila Rift 587 This equation shows that the ratio EV K =EY V varies from 3.4 for A-type stars to 3.6 for K− giants.− Since the∼ ratio ∼ EY V =EB V 0:8forAstarsand 0.85 for K giants, − − ≈ ≈ Eq.
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